| DOI | Trouver le DOI : https://doi.org/10.1093/mnras/stad887 |
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| Auteur | Rechercher : Sokolovsky, K VIdentifiant ORCID : https://orcid.org/0000-0001-5991-6863; Rechercher : Johnson, T JIdentifiant ORCID : https://orcid.org/0000-0002-2771-472X; Rechercher : Buson, SIdentifiant ORCID : https://orcid.org/0000-0002-3308-324X; Rechercher : Jean, PIdentifiant ORCID : https://orcid.org/0000-0002-1757-9560; Rechercher : Cheung, C CIdentifiant ORCID : https://orcid.org/0000-0002-4377-0174; Rechercher : Mukai, KIdentifiant ORCID : https://orcid.org/0000-0002-8286-8094; Rechercher : Chomiuk, LIdentifiant ORCID : https://orcid.org/0000-0002-8400-3705; Rechercher : Aydi, EIdentifiant ORCID : https://orcid.org/0000-0001-8525-3442; Rechercher : Molina, B; Rechercher : Kawash, AIdentifiant ORCID : https://orcid.org/0000-0003-0071-1622; Rechercher : Linford, J DIdentifiant ORCID : https://orcid.org/0000-0002-3873-5497; Rechercher : Mioduszewski, A J; Rechercher : Rupen, M P1; Rechercher : Sokoloski, J L; Rechercher : Williams, M N; Rechercher : Steinberg, EIdentifiant ORCID : https://orcid.org/0000-0003-0053-0696; Rechercher : Vurm, IIdentifiant ORCID : https://orcid.org/0000-0003-1336-4746; Rechercher : Metzger, B DIdentifiant ORCID : https://orcid.org/0000-0002-4670-7509; Rechercher : Page, K LIdentifiant ORCID : https://orcid.org/0000-0001-5624-2613; Rechercher : Orio, MIdentifiant ORCID : https://orcid.org/0000-0003-1563-9803; Rechercher : Quimby, R MIdentifiant ORCID : https://orcid.org/0000-0001-9171-5236; Rechercher : Shafter, A WIdentifiant ORCID : https://orcid.org/0000-0002-1276-1486; Rechercher : Corbett, HIdentifiant ORCID : https://orcid.org/0000-0002-6339-6706; Rechercher : Bolzoni, SIdentifiant ORCID : https://orcid.org/0000-0003-0114-1318; Rechercher : DeYoung, J; Rechercher : Menzies, K; Rechercher : Romanov, F DIdentifiant ORCID : https://orcid.org/0000-0002-5268-7735; Rechercher : Richmond, M; Rechercher : Ulowetz, J; Rechercher : Vanmunster, T; Rechercher : Williamson, G; Rechercher : Lane, D JIdentifiant ORCID : https://orcid.org/0000-0002-6097-8719; Rechercher : Bartnik, M; Rechercher : Bellaver, M; Rechercher : Bruinsma, E; Rechercher : Dugan, E; Rechercher : Fedewa, J; Rechercher : Gerhard, C; Rechercher : Painter, S; Rechercher : Peterson, D-M; Rechercher : Rodriguez, J EIdentifiant ORCID : https://orcid.org/0000-0001-8812-0565; Rechercher : Smith, C; Rechercher : Sullivan, H; Rechercher : Watson, S |
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| Affiliation | - Conseil national de recherches du Canada. Herzberg en astronomie et en astrophysique
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| Bailleur de fonds | Rechercher : National Aeronautics and Space Administration; Rechercher : Ministry of Education, Culture, Sports, Science and Technology; Rechercher : Japan Aerospace Exploration Agency; Rechercher : Swedish Research Council; Rechercher : Istituto Nazionale di Astrofisica; Rechercher : DOE; Rechercher : National Science Foundation |
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| Format | Texte, Article |
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| Sujet | stars: individual: V1674 Her; novae; cataclysmic variables; white dwarfs; transients: novae |
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| Résumé | Classical novae are shock-powered multiwavelength transients triggered by a thermonuclear runaway on an accreting white dwarf. V1674 Her is the fastest nova ever recorded (time to declined by two magnitudes is t2 = 1.1 d) that challenges our understanding of shock formation in novae. We investigate the physical mechanisms behind nova emission from GeV γ-rays to cm-band radio using coordinated Fermi-LAT, NuSTAR, Swift, and VLA observations supported by optical photometry. Fermi-LAT detected short-lived (18 h) 0.1–100 GeV emission from V1674 Her that appeared 6 h after the eruption began; this was at a level of (1.6 ± 0.4) × 10⁻⁶ photons cm⁻² s⁻¹. Eleven days later, simultaneous NuSTAR and Swift X-ray observations revealed optically thin thermal plasma shock-heated to kTshock = 4 keV. The lack of a detectable 6.7 keV Fe Kα emission suggests super-solar CNO abundances. The radio emission from V1674 Her was consistent with thermal emission at early times and synchrotron at late times. The radio spectrum steeply rising with frequency may be a result of either free-free absorption of synchrotron and thermal emission by unshocked outer regions of the nova shell or the Razin–Tsytovich effect attenuating synchrotron emission in dense plasma. The development of the shock inside the ejecta is unaffected by the extraordinarily rapid evolution and the intermediate polar host of this nova. |
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| Date de publication | 2023-03-23 |
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| Maison d’édition | Oxford Academic |
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| Dans | |
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| Langue | anglais |
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| Publications évaluées par des pairs | Oui |
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| Exporter la notice | Exporter en format RIS |
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| Signaler une correction | Signaler une correction (s'ouvre dans un nouvel onglet) |
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| Identificateur de l’enregistrement | 6b882c14-2bd7-434e-861d-9667ff82a8dd |
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| Enregistrement créé | 2024-06-27 |
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| Enregistrement modifié | 2024-06-27 |
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